SSL UC Berkeley 2010 June ACE/SOHO/STEREO/Wind Workshop Interplanetary Propagation of Solar Impulsive Energetic Electrons Linghua Wang, Bob Lin and S ä m Krucker Space Sciences Lab, UC Berkeley

F Summary for the five events * Two different PAD behaviors at low and high energies: At low energies (~0.3keV to E 0 ), the PAHM remains roughly constant below 30° (corresponding to an actual PAHM of <~15°, limited by the instrumental response) from onset through the peak. At high energies (E 0 to ~300 keV), the PAHM increases with energy, e.g., from ~30° at E 0 up to 85° at 300 keV at the peak; it also increases with time. The energy transition E 0 varies from ~10 to 30 keV, from event to event. ρ e = ρ Tp

F * Although the energy transition E 0 varies from ~10 to 30 keV and the Tp varies from ~7 to 33 eV, the E 0 always corresponds to a ρ e0 ~ ρ Tp. The ratio Λ of the peak flux of outward-traveling scattered electrons to field-aligned scatter- free electrons Summary for the five events

F The ratio Λ of the peak flux of outward-traveling scattered electrons to field-aligned scatter- free electrons Summary for the five events At energies with ρ e > ρ Tp, electrons would scatter more due to stronger power densities for fluctuations/waves at scale λ > ρ Tp (the inertial range), and the power-law increase of Λ with ρ e may be associated with the power-law increase of turbulence power density with λ (P  λ β ). At energies with ρ e < ρ Tp, electrons would be weakly scattered because of weak power densities for resonant fluctuations/waves at scale λ < ρ Tp (the dissipation range).

F * For high-energy electrons, the observed flux-time profiles retain a rapid-rise, rapid-decay peak and the estimated path length is only ~4-18% longer than the smooth spiral field length, indicating that strong scattering, if it existed within 1 AU, only occurred near 1 AU since strong scattering (mean free path 4hours for mean free path <~ 0.4 AU) peak [Lin, 1974] and a much larger path length. Such propagation cannot explain the previously reported delay of ~10-30 min for high-energy electrons [Krucker et al., 1999; Haggerty & Roelof, 2002; Wang et al., 2006]. Thus, this delay must reflect the actual delay in the solar injection of high-energy electrons. Summary for the five events